The Galactic microquasar GRS 1716–249 (or GRO J1719–24 or Nova Oph 1993) was first detected on 1993 September 25, independently and simultaneously by the BATSE instrument aboard CGRO [1]} and the SIGMA telescope aboard GRANAT [2]}. The optical counterpart was discovered by [3]} and [4]}, as a low mass main-sequence star of spectral type K (or later). The mass of the companion is star found to be \(\sim 1.6 M_\odot \) , and the system has an orbital period of \(\sim \)  14.7 hr. The compact object is believed to be a stellar-mass black hole of mass \(\sim 4.9 M_\odot \) , located at a distance of \(\sim \)  2.0–2.8 kpc. The only observed historical major outburst from GRS 1716–249 coincided with its discovery in 1993, which was later studied in detail by [5]}, to investigate the nature of its temporal variability. During the entire 80 days of its outburst, the authors witnessed a QPO at \(\nu \sim \)  0.04 Hz at the beginning of the observations, which gradually shifted to 0.3 Hz at the end. A constant phase lag of \(0.072\pm 0.010\)  radian was also observed in the frequency range 0.02\(-\) 0.20 Hz. [6]} observed that the \(\le \)  1 Hz QPO was similar to type II burst profiles of Rapid Bursters associated with neutron star accretors. This variability feature suggests that the origin of the \(\le \)  1 Hz QPO is independent of the nature of the accretor, and the \(\sim \)  0.04 Hz QPO originates from thermal viscous instabilities in the accretion disk surrounding the black hole.
